Python I, II, and III cosmic microwave background anisotropy measurement constraints on open and flat-A cold dark matter cosmogonies

We use Python I, II, and III cosmic microwave background anisotropy data to constrain cosmogonies. We account for the Python beamwidth and calibration uncertainties. We consider open and spatially flat-Lambda cold dark matter cosmogonies, with nonrelativistic mass density parameter Omega(0) in the r ange 0.1-1, baryonic mass density parameter Omega(B), in the range (0.005-0 .029) h(-2), and age of the universe t(0) in the range (10-20) Gyr. Margina lizing over all parameters but Omega(0), the combined Python data favor an open (spatially flat-Lambda) model with Omega(0) similar or equal to 0.2 (0 .1). At the 2 sigma confidence level, model normalizations deduced from the combined Python data are mostly consistent with those drawn from the DMR, UCSB South Pole 1994, ARGO, MAX 4 and 5, White Dish, and SuZIE data sets.